6. THE INFLUENCE OF SUPERNOVAE

After a burst of star formation has taken place, the first supernovae appear
after about 10 million years. These Type II supernovae arise from collapsing
massive stars which have exhausted most of their nuclear fuel. Type II
supernovae are distributed like the young stars in a disk galaxy, i.e.
concentrated along spiral arms.
A billion years after the initial starburst, the Type I supernovae appear.
Type Ia supernovae are thought to be due to accretion of matter by a white
dwarf in a binary pair. These are to be found among the older stellar
population and therefore have an exponential distribution with radius like the
underlying disk.

The increase in Type Ia supernovae towards the Galactic centre implies that
here the ISM likely
becomes supernova-dominated, resulting in a two phase ISM with only an
HIM and a CNM. The warm phases are disrupted as diffuse clouds are shocked and
heated to high temperatures. The molecular clouds survive the assault of
supernovae and remain essntially intact, having only their outer warm layers
stripped away. The scale height of the oldest stellar populations is higher
(~ 300 pc) than for the atomic hydrogen (~ 100 pc), such that
half of all Type Ia supernovae explode above the gas and therefore deposit much
of their energy directly to the halo. This picture produces a volume filling
fraction of about 25% for the HIM, and presumably explains the HI holes seen
in external galaxies.

The correlated distribution of Type II supernovae has an important consequence.
The time interval between successive supernovae is less than the bubble
lifetime.
This can result in a large-scale wind of energy into the Galactic halo. Heiles
(1987) derives a two-dimensional porosity parameter

(2)

where is the supernova rate in
kpc-2
Myr-1, s (~ 2)
is a correlation factor, and N (~ 40) is the number of Type II
supernovae that
occur in a single association. But this leads to a volume filling factor
of more
than 95% along the spiral arms, and about 80% outside of the arms, contrary
to observation. Furthermore, the Type II energy flow is expected to break out
and produce a mass flow rate of ~ 20
M per year,
which would
deplete the total gas content of the disk in 109 yr. How are we to
reconcile this?